Many aspects of nuclear matter are reflected in the relationship between the mass and radius of neutron stars. The radius of a neutron star is mainly determined by its mass and the nuclear matter equation of state
(EOS), in addition to some other factors such as spin [1]}. This means simultaneous observations of neutron star masses and radii, i.e., mass-radius measurements, can be inverted to deduce the nuclear EOS. The fact that the EOS has not been computed from first principles with high accuracy due to the nonperturbative nature of quantum chromodynamics, especially for higher nucleon densities, makes this astrophysical strategy all the more valuable [2]}, [3]}.
